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We thank the referee for his/her useful comments, that helped improve this manuscript. TH acknowledges Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Argentina, for their supporting fellowships. AO acknowledges support from project AYA2015-66211-C2-2 of the Spanish Ministerio de Economia, Industria y Competitividad. SAC acknowledges funding from CONICET (PIP-0387), and Universidad Nacional de La Plata (G11-150), Argentina. This project has received funding from the European Union's Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie grant agreement No. 734374; project acronym: LACEGAL. The programmes and figures had been developed under PYTHON language (Van Rossum & Drake 2009), using specially NUMPY (Van Der Walt, Colbert & Varoquaux 2011) and MATLOTLIB (Hunter 2007).

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Are Ly alpha emitters segregated in protoclusters regions?

Publicado en:MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 499 (2): 2104-2115 - 2020-12-01 499(2), DOI: 10.1093/mnras/staa3027

Autores: Hough, Tomas; Gurung-Lopez, Siddhartha; Orsi, Alvaro; Cora, Sofia A.; Lacey, Cedric G.; Baugh, Carlton M.;

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The presence of neutral hydrogen in the interstellar medium (ISM) and intergalactic medium (IGM) induces radiative transfer (RT) effects on Ly alpha photons that affect the observability of Lyman alpha emitters (LAEs). We use the GALFORM semi-analytic model of galaxy formation and evolution to analyse how these effects shape the spatial distribution of LAEs with respect to H alpha emitters (HAEs) around high-density regions at high redshift. We find that when a large sample of protoclusters is considered, HAEs showing also Ly alpha emission (HAEs + LAEs) populate the same regions as those that do not display the Ly alpha line at z = 2.2. We compare against the protocluster USS1558-003, one of the most massive protoclusters located at z = 2.53. Our results indicate that the strong depletion of HAEs + LAEs present in the high-density regions of USS1558-003 may be due to cosmic variance. We find that at z = 2.2 and z = 3.0, RT of the ISM produces a strong decline (30-50 per cent) of the clustering amplitude of HAEs + LAEs with respect to HAEs towards the protoclusters centre. At z = 5.7, given the early evolutionary state of protoclusters and galaxies, the clustering of HAEs + LAEs has a smaller variation (10-20 per cent) towards the protoclusters centre. Depending on the equivalent width and luminosity criteria of the emission-line galaxy sample, the IGM can have a mild or a null effect on galaxy properties and clustering in high-density regions.

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